Therefore, the accretion rate onto PDS 70 b is likely \(\dot{M} \approx 2\times 10^{-7}\) –\(10^{-4}~M_{\mathrm {J}}\,\mathrm {yr}^{-1}\) . This large spread folds in the uncertainties on the accretion geometry. The results are very similar for \(M_{\mathrm {p}}=3~M_{\mathrm {J}}\)  or the Cold radius function instead (not shown).
This range of \(\dot{M}\)  is higher than \(\dot{M} =10^{-8}~M_{\mathrm {J}}\,\mathrm {yr}^{-1}\)  as derived by [1]}, but that was based on a low-mass extrapolation of empirical correlations for stars.
[2]} found that it is invalid at low masses,
as can also be seen in Figure REF 
from the discrepancy between the [3]} correlation for CTTSs and our curves.
